2006/02/27 by J. de Plaa, N. Werner, A. M. Bykov +7 · 93 citations
Engineering · Physics and Astronomy · #Astronomy and Astrophysical Research #Cluster (spacecraft) #Cosmic microwave background #Galaxies: Formation, Evolution, Phenomena #Galaxy #Galaxy cluster #Line (geometry) #Metallicity #Space Technology and Applications #Spectral line #Star formation #Stars #astro-ph
paper · pdf · doi:10.1051/0004-6361:20053864
published in Astronomy and Astrophysics 452(2), 397-412 (EDP Sciences) · 18 pages, 11 figures, Accepted for publication in Astronomy & Astrophysics
arxiv created 2006/02/27 · openalex publication_date 2006/05/22 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
Using a new long X-ray observation of the cluster of galaxies Sérsic 159-03 with XMM-Newton, we derive radial temperature and abundance profiles using single- and multi-temperature models. The fits to the EPIC and RGS spectra prefer multi-temperature models especially in the core. The radial profiles of oxygen and iron measured with EPIC/RGS and the line profiles in RGS suggest that there is a dip in the O/Fe ratio in the centre of the cluster compared to its immediate surroundings. A possible explanation for the large scale metallicity distribution is that SNIa and SNII products are released in the ICM through ram-pressure stripping of in-falling galaxies. This causes a peaked metallicity distribution. In addition, SNIa in the central cD galaxy enrich mainly the centre of the cluster with iron. This excess of SNIa products is consistent with the low O/Fe ratio we detect in the centre of the cluster. We fit the abundances we obtain with yields from SNIa, SNII and Population-III stars to derive the clusters chemical evolution. We find that the measured abundance pattern does not require a Population-III star contribution. The relative contribution of the number of SNIa with respect to the total number of SNe which enrich the ICM is about 25-50%. Furthermore, we discuss the possible presence of a non-thermal component in the EPIC spectra. A potential source of this non-thermal emission can be inverse-Compton scattering between Cosmic Microwave Background (CMB) photons and relativistic electrons, which are accelerated in bow shocks associated with ram-pressure stripping of in-falling galaxies.